烃源岩—流体相互作用模拟实验研究

为了探讨烃源岩与孔隙流体之间相互作用过程和机理以及有机酸的生成及其影响因素,我们开展了烃源岩-流体相互作用模拟实验研究。实验结果表明：Ⅱ型干酪根形成有机酸的能力大于Ⅰ型干酪根,水的矿化度对有机酸的形成影响甚微,随着温度升高,流体中有机酸的含量也随之增大。pH值对有机酸形成的影响非常明显,中性和碱性条件更有利于生成有机酸。其中乙酸的形成有利于碳酸盐矿物的溶解,而草酸的形成不利于碳酸盐的溶解。温度对烃源岩的影响与烃源岩的矿物组成有很大的关系,对于富碳酸盐烃源岩,Ca、Mg、Na三元素在水中的溶解量,与温度呈反相关的关系,对于贫碳酸盐烃源岩,与反应温度之间则呈现出正相关的关系。而无论碳酸盐含量高低,Si在溶液中的含量都会随着温度的升高而增大。酸性溶液对烃源岩的溶解能力最强,无论原始反应溶液的酸碱性,反应结果都最终趋于弱碱性。流体的含盐量对烃源岩中Mg的溶解影响差异较大,低盐度的流体有利于Mg溶解。     

云南金顶铅锌矿床的有机成矿作用——来自围岩、矿石中有机质生物标志化合物的证据

云南金顶铅锌矿床是世界上成矿时代最新且唯一的陆相沉积岩容矿的超大型铅锌矿床。矿区存在2类有机质——原生型和迁移型,与矿石共生。生物标志化合物研究结果表明：正构烷烃碳数分布范围较宽,有2种峰型;萜烷化合物的相对丰度五环三萜烷＞三环萜烷＞四环萜烷;规则甾烷C27～C28～C29呈不对称V字型分布;有机质的母质来源以低等水生生源的海藻类为主,伴随有一定量的陆源高等植物组分;有机质沉积于弱氧化—弱还原环境;成矿热液的热力作用使样品遭受了一定程度的热解,部分样品还遭受了生物降解作用;生物标志物多参数对比表明有机质来源于三叠纪三合洞组碳酸盐岩地层。原生型有机质的成矿作用主要体现在对成矿金属元素的预富集上,而迁移型有机质的成矿作用主要是对成矿金属元素的活化运移。     

加水热模拟中深湖与煤系泥岩地化特征比较

通过深湖泥岩和煤系泥岩的加水热模拟研究认为,在热模拟实验过程中,深湖泥岩和煤系泥岩显示不同特征,并且其演化有差别。深湖泥岩利于液态原油的生成,并且转化率高于煤系泥岩。深湖泥岩残余可溶有机质饱和烃含量高于煤系泥岩,非烃含量则低于煤系泥岩。深湖泥岩胶质 /沥青质和饱芳比均随温度升高而降低,而煤系泥岩的胶质 /沥青质随温度升高有增加趋势,其饱芳比的变化则不大或有降低趋势。深湖泥岩的T_max难以指示演化阶段,其干酪根碳同位素值明显轻于煤系泥岩,它们的值均随温度的升高而变重。     

Dust and gas in W49A

We have mapped the high-mass star-forming region W49A at 450, 800, and 1100 microns with the JCMT. Spectral index measurements suggest an increase in temperature towards the emission peaks, consistent with previous data. We derive the gas masses associated with the central and extended emission from each of the three components, and find a deficit of gas around W49SW. The mass found for the core of W49N is in good agreement with the value previously derived from C³⁴S (5-4) maps (Serabynet al., 1993), and similar morphologies are found in the line and continuum maps.     

暗物质粒子探测器触发逻辑测试系统的设计和实现?

作为暗物质粒子探测器(DAMPE, Dark Matter Particle Explorer)的一部分,触发系统主要用于判选所需探测的目标粒子(高能电子和伽玛射线)事例,剔除非目标粒子事例。触发系统由触发探测器和触发判选逻辑电路组成。介绍了触发地检测试系统和宇宙线触发系统的设计和功能实现。触发地检系统实现了对触发判选逻辑电路的电子学验证;另外,配合宇宙线触发系统对部分触发逻辑和触发效率进行了测试。主要介绍了触发系统的测试方法和一些初步测试结果。     

Molecules as probes of star-forming regions (Review)

This paper is a brief review of molecular spectroscopy methods for the diagnostics of star-forming regions. Principal attention is paid to the determination of the kinetic temperature and gas density in dense clouds, the radiation field temperature, the magnetic field, and the spatial and velocity structure of regions of star formation.     

Magnetic draping of merging cores and radio bubbles in clusters of galaxies

Sharp fronts observed by the Chandra satellite between dense cool cluster cores moving with near-sonic velocity through the hotter intergalactic gas, require strong suppression of thermal conductivity across the boundary. This may be due to magnetic fields tangential to the contact surface separating the two plasma components. We point out that a super-Alfvenic motion of a plasma cloud (a core of a merging galaxy) through a weakly magnetized intercluster medium leads to 'magnetic draping', formation of a thin, strongly magnetized boundary layer with a tangential magnetic field. For supersonic cloud motion,   M _s≥ 1  , magnetic field inside the layer reaches near-equipartition values with thermal pressure. Typical thickness of the layer is  ∼ L / M ²_A≪ L   , where L is the size of the obstacle (plasma cloud) moving with Alfvén Mach number   M _A≫ 1  . To a various degree, magnetic draping occurs for both subsonic and supersonic flows, random and ordered magnetic fields and it does not require plasma compressibility. The strongly magnetized layer will thermally isolate the two media and may contribute to the Kelvin–Helmholtz stability of the interface. Similar effects occur for radio bubbles, quasi-spherical expanding cavities blown up by active galactic nucleus jets; in this case, the thickness of the external magnetized layer is smaller,  ∼ L / M ³_A≪ L   .     

On the Dynamics of Dust Grains in a Hierarchical Environment

Most main sequence stars are binaries or higher multiplicity Systems and it appears that at birth most stars have circumstellar disks. It is commonly accepted that planetary systems arise from the material of these disks; consequently, binary and multiple systems may have a main role in planet formation. In this paper, we study the stage of planetary formation during which the particulate material is still dispersed as centimetre-to-metre sized primordial aggregates. We investigate the response of the particles, in a protoplanetary disk with radius R_D = 100 AU around a solar-like star, to the gravitational field of bound perturbing companions in a moderately wide (300–1600 AU) orbit. For this purpose, we have carried out a series of simulations of coplanar hierarchical configurations using a direct integration code that models gravitational and viscous forces. The massive protoplanetary disk is around one of the components of the binary. The evolution in time of the dust sub-disk depends mainly on the nature (prograde or retrograde) of the relative revolution of the stellar companion, and on the temperature and mass of the circumstellar disk. Our results show that for binary companions near the limit of tidal truncation of the disk, the perturbation leads to an enhanced accretion rate onto the primary, decreasing the lifetime of the particles in the protoplanetary disk with respect to the case of a single star. As a consequence of an enhanced accretion rate the mass of the disk decreases faster, which leads to a longer resultant lifetime for particles in the disk. On the other hand, binary companions may induce tidal arms in the dust phase of protoplanetary disks. Spiral perturbations with m = 1 may increase in a factor 10 or more the dust surface density in the neighbourhood of the arm, facilitating the growth of the particles. Moreover, in a massive disk (0.01M⊙) the survival time of particles is significantly shorter than in a less massive nebula (0.001M⊙) and the temperature of the disk severely influences the spiral-in time of particles. The rapid evolution of the dust component found in post T Tauri stars can be explained as a result of their binary nature. Binarity may also influence the evolution of circumpulsar disks. This revised version was published online in July 2006 with corrections to the Cover Date.     

Relative molar mass distributions of chromophoric colloidal organic matter in coastal seawater determined by Flow Field-Flow Fractionation with UV absorbance and fluorescence detection

A new method for the characterization of chromophoric colloidal organic matter in seawater has been applied to samples from the Baltic Sea, Kattegatt and Skagerrak seas. Size fractionation of the sample by Flow Field-Flow Fractionation and measurement of the fluorescent and UV absorbing properties of the individual size fractions result in a relative molar mass distribution (RMM) of the optical properties. The RMM distributions have been used to estimate number and weight average relative molar masses, and polydispersity indices. At least two sources of coloured organic matter were identified from the ratio of fluorescence to UV: the Baltic surface water and the Skagerrak deep water. The dominating processes were mixing and dilution, but processes such as photo bleaching of fluorescence are also believed to be important. The RMM distribution derived from UV detection (1150–1300 Dalton) increased with increasing salinity while that derived for fluorescence (1500–1250 Dalton) decreased with increasing salinity. The specific UV absorbance taken as a proxy of the aromaticity of the chromophoric organic material showed decreasing trend with both increasing salinity and increasing UV derived weight average relative molar mass. Increasing polydispersity of the colloidal material was also observed as a function of salinity.